Interstellar clouds and molecular hydrogen

Details Interstellar clouds and molecular hydrogen Interstellar clouds and molecular hydrogen

Aug 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977amsci..65..446j&link_type=abstract

American Scientist, vol. 65, July-Aug. 1977, p. 446-454. NASA-NSF-supported research.

Astronomy and Astrophysics

Astronomy

Hydrogen Clouds, Interstellar Gas, Oao 3, Optical Thickness, Absorption Spectra, Cosmic Dust, Gas Density, Luminosity, Nebulae, Stellar Evolution, Ubv Spectra

Scientific paper

Data obtained from the Copernicus Orbiting Astronomical Observatory, launched in 1972 and still obtaining information, are used in a discussion of the interstellar medium. The Copernicus instruments have facilitated direct estimates for the density and temperature of individual interstellar clouds, and improved the ability to determine where along the line of sight a cloud lies with respect to background stars. The physical characteristics of hydrogen molecules are considered, with attention to the formation and destruction of interstellar hydrogen. The differences between 'thin' clouds, in which molecular hydrogen is optically thin, and 'thick' clouds are examined. Several features of the interstellar medium are described.

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